with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed am initial weak peak
near the trigger time followed by stronger emission starting about 100
seconds later. The total duration is about 150 sec. The peak count rate
was ~4500 counts/sec (15-350 keV), at ~135 sec after the trigger.
The XRT began observing the field at 09:50:58.0 UT, 74.4 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
298.8244, -67.7029 which is equivalent to:

RA(J2000) = 19h 55m 17.85s
Dec(J2000) = -67d 42' 10.6"

with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 44 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.
A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (6.49 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 5.3
(+2.89/-2.47) x 10^21 cm^-2 (90% confidence).
The initial flux in the 2.5 s image was 4.69e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 82 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag.
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.10.
Burst Advocate for this burst is E. Troja (eleonora.troja AT nasa.gov).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)

with an uncertainty of 1.7 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.

with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 43%.
The mask-weighted light curve shows a complex structure. The first set of peaks
begins around T-10 sec, peaks at T+2 and fades by T+10 sec. The second set
of peaks begins around T+92 sec, peaks at T+102 sec and fades nearly to
background by T+115 sec. This is when the third set of peaks begins to rise,
which peaks at T+T+135 sec and fades by T+160 sec. All of these peak
structures have multiple sub-peaks. T90 (15-350 keV) is 152.51 +- 3.37 sec
(estimated error including systematics).
The time-averaged spectrum from T-8.32 to T+157.44 sec is best fit by a power law
with an exponential cutoff. This fit gives a photon index 1.39 +- 0.28,
and Epeak of 37.5 +- 5.5 keV (chi squared 39.62 for 56 d.o.f.). For this
model the total fluence in the 15-150 keV band is 6.0 +- 0.2 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+133.80 sec in the 15-150 keV band is
6.0 +- 0.3 ph/cm2/sec. A fit to a simple power law gives a photon index
of 2.14 +- 0.06 (chi squared 64.42 for 57 d.o.f.). All the quoted errors
are at the 90% confidence level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/722642/BA/